jats:titleAbstract</jats:title> jats:pWe study spatially resolved scaling relations among stars, dust, and gas in ten nearby spiral galaxies. In a preceding paper, we have derived spatially resolved properties of the stellar population and dust by a panchromatic spectral energy distribution fitting using jats:monospacepiXedfit</jats:monospace>. Now, we investigate resolved star formation (jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow <mml:mi mathvariant="normal">Σ</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>–Σjats:subSFR</jats:sub>–Σjats:sub*</jats:sub>) and dust scaling relations. While the relations with all subgalactic regions of the galaxies are reasonably tight (jats:italicσ</jats:italic> ≲ 0.3 dex), we find that most of the scaling relations exhibit galaxy-to-galaxy variations in normalization and shape. Only two relations of Σjats:subdust</jats:sub>–Σjats:subgas</jats:sub> and Σjats:subdust</jats:sub>–jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow <mml:mi mathvariant="normal">Σ</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> do not show noticeable galaxy-to-galaxy variations among our sample galaxies. We further investigate the correlations among the scaling relations. We find significant correlations among the normalization of the jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow <mml:mi mathvariant="normal">Σ</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>–Σjats:subSFR</jats:sub>–Σjats:sub*</jats:sub> relations, which suggest that the galaxies with higher levels of resolved Hjats:sub2</jats:sub> fraction (jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow mml:mif</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn4.gif" xlink:type="simple" /> </jats:inline-formula>) tend to have higher levels of resolved star formation efficiency (SFE) and specific star formation rate (sSFR). We also observe that the galaxies with higher levels of resolved dust-to-stellar mass ratios tend to have higher levels of resolved sSFR, SFE, and jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow mml:mif</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn5.gif" xlink:type="simple" /> </jats:inline-formula>. Moreover, we find that the galaxies with higher global sSFR and less compact morphology tend to have higher levels of the resolved sSFR, SFE, and jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow mml:mif</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn6.gif" xlink:type="simple" /> </jats:inline-formula>, which can explain the variations in the normalization of the jats:inline-formula jats:tex-math

</jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> mml:msub mml:mrow <mml:mi mathvariant="normal">Σ</mml:mi> </mml:mrow> mml:mrow mml:msub mml:mrow <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> mml:mrow mml:mn2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac7da4ieqn7.gif" xlink:type="simple" /> </jats:inline-formula>–Σjats:subSFR</jats:sub>–Σjats:sub*</jats:sub> relationships. Overall, we observe indications of the contributions of both global and local factors in governing the star formation process in galaxies.</jats:p>